Host Optical Cutout
0.26″/pix
DESI DR10 Optical (0.26″/pix)
Core Parameters
| R.A. (J2000) | 01:18:46.498 (19.69374°) |
|---|---|
| Dec. (J2000) | +14:59:30.57 (14.99182°) |
| Spectral Type | II |
| Redshift (z) | 0.022751 |
| Recession Velocity | 6,743 km/s (redshift Doppler-equivalent) |
| Luminosity Distance | 99.14 Mpc (~323.4 Million Light-Years, μ = 34.98) |
| Peak Apparent Mag | 18.93 ± 0.11 (i) brightest multi-epoch detection (2026/10/05 (MJD 61318.3)) |
| Peak Absolute Mag | -16.05 mag (-16.19 mag (A_V corrected)) |
| MW Dust E(B-V) | 0.0451 mag (AV = 0.14 mag) derived from galactic coordinates (Analytical Galactic Disk Model (IAU)), not a dust-map measurement |
| Host Galaxy | — |
| Host Offset | — |
| Observations | 11 detections, 1 spectra |
Interactive Sky Field (Aladin) ✨ DSS2 Optical (China-VO mirror)
🎯 01:18:46.498 +14:59:30.57
FOV: 0.15°
● SN2026abur (II)
Coordinate Pointing & Airmass
Discovered 60 days ago (2026/09/14). Cataloged peak 2026/10/05 (MJD 61318.3) (39d ago; rest-frame phase +38.1d). Cataloged/observed peak: m = 18.93 on 2026/10/05 (MJD 61318.3). Latest observed: m = 19.30 on 2026/10/07 (MJD 61320.3). No reliable current brightness estimate — no event-specific brightness fit with documented uncertainty is published for this object. Class-average decay templates are not used as object-specific predictions. Latest observed magnitude: m = 19.30 on 2026/10/07 (MJD 61320.3). Current brightness trend is unknown (last observation 2026/10/07 (MJD 61320.3); same-band recent pair unavailable or stale). Use the window below to plan observations tonight.
Multi-Band Light Curve
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Calibrated Spectra Viewer
🌌 Cosmic Neighbors & Contemporaries
105,868+ transients indexed
Cataloged transients closest to SN2026abur in discovery time, spatial sky neighborhood, and cosmological redshift:
⏱️ Closest in Time
SN2026ahyg
+17d after
Type IIP
2026/10/01 · Mag 19.2701
SN2026afqb
+21d after
Type Ia
2026/10/05 · Mag 20.6842
SN2026aevi
+22d after
Type Ia
2026/10/06 · Mag 19.99
Literature & Data Provenance
| ID | Source | Reference | NASA ADS Bibcode |
|---|---|---|---|
| [1] | Transient Name Server | — | |
| [2] | 2026TNSTR3742....1M | ZTFReST_bot | 2026TNSTR3742....1M |
| [3] | The Open Supernova Catalog | Guillochon et al. (2017) | 2017ApJ...835...64G |
| [4] | ALeRCE / ZTF | — |
❓ Frequently Asked Questions About SN2026abur
Scientific & observational Q&As indexed from astronomical databases & the sne.space
What type of supernova is SN2026abur and what kind of star exploded? Astrophysics & Progenitor
SN2026abur is classified as a Type II supernova, consistent with core collapse of a massive star that retained hydrogen in its outer envelope. Typical progenitor mass ranges quoted for the class are model expectations, not a measured mass for this star.
What was the progenitor star doing in the millions of years leading up to SN2026abur? Astrophysics & Progenitor
The specific progenitor of SN2026abur has not been observed. Events of this spectroscopic class are generally associated with massive-star core collapse after successive nuclear burning stages (hydrogen → helium → carbon → neon → oxygen → silicon → iron). Typical lifetimes of such progenitors are tens of millions of years, but that is a class expectation—not a measured age or evolutionary track for this star. No pre-explosion imaging identification is cited in the available record for SN2026abur.
How far away is SN2026abur from Earth and how old is the light reaching us? Cosmic Distance & Time
SN2026abur has a luminosity distance of approximately 323.4 Million Light-Years (redshift z = 0.022751, d_L = 99.14 Mpc). Under a flat ΛCDM cosmology (H₀≈70 km/s/Mpc, Ωₘ≈0.3), the corresponding lookback time is ≈313 Myr — when the light set out 312.6 million years ago during the Paleozoic era, long before the first dinosaurs appeared on Earth. Luminosity distance is larger than the light-travel distance because cosmic expansion stretches the path; the two must not be equated.
What does the cosmological redshift of SN2026abur tell us about the expansion of space? Cosmic Distance & Time
SN2026abur exhibits a measured spectroscopic redshift of z = 0.0228. The cockpit reports a user-facing recession velocity of 6,743.0 km/s, computed as the redshift Doppler-equivalent v = c·((1+z)²−1)/((1+z)²+1). Cosmological redshift is not generally equivalent to special-relativistic motion through space; this number is a convenient velocity label for z, not a measured peculiar velocity and not supernova ejecta speed. Bare c·z (≈6,821 km/s) is a different low-z approximation and is not mixed here.
How bright did SN2026abur become at its peak, and how many Suns does that equal? Explosion Energetics
At peak brightness, SN2026abur achieved an apparent magnitude of 18.93 ± 0.11 (i) around 2026/10/05 (MJD 61318.3). Corrected for cosmic distance and foreground interstellar dust, its intrinsic absolute magnitude was -16.05 mag. At this peak, the exploding star radiated with the incandescent brilliance of approximately 224.9 million Suns combined, briefly outshining the cumulative starlight of entire dwarf galaxies!
How much total energy was released by SN2026abur, and where did that energy go? Explosion Energetics
Core-collapse events of this broad class are often discussed with a ~10⁵³ erg gravitational binding energy of which ~99% may escape as neutrinos—again a class scale, not a measured budget for SN2026abur.
How fast are the supernova ejecta and shockwave of SN2026abur expanding through space? Explosion Energetics
No ejecta velocity is measured for SN2026abur. Blast-wave speed is obtained from Doppler shifts of spectral absorption features (e.g. Si II λ6355 for Type Ia), not from cosmological redshift. Any recession velocity derived from z describes Hubble flow, not the explosion debris. Type II events typically show ejecta speeds of order ~8,500 km/s near maximum, but that class scale is not a measurement of SN2026abur.
What powers the prolonged glow of SN2026abur weeks and months after detonation? Radioactive Engine
Classified core-collapse light curves are often sustained after peak by radioactive ⁵⁶Ni → ⁵⁶Co → ⁵⁶Fe decay, with typical nickel yields of order 0.05–0.15 solar masses—again a class scale, not a measured yield for SN2026abur. Shock-breakout heating may dominate the earliest optical flash; without a published bolometric fit, neither nickel mass nor the dominant power source is established for this event.
What chemical elements did SN2026abur create and disperse into the universe? Nucleosynthesis & Elements
Events of SN2026abur's broad spectroscopic class are discussed in galactic chemical evolution as sources of oxygen-group and intermediate-mass elements (and, for some channels, iron-peak material). No measured elemental yields are published for SN2026abur.
Did SN2026abur leave behind a black hole, a neutron star, or nothing at all? Cosmic Remnant
A core-collapse explosion associated with SN2026abur's class forges an ultra-dense compact stellar remnant at the center of the detonation. If the progenitor had an initial mass under ~20 solar masses, it left behind a neutron star (pulsar)—packing the mass of our entire Sun into a city-sized sphere barely 20 kilometers wide, spinning dozens or hundreds of times per second. If the progenitor exceeded ~25–30 solar masses, gravity overcame neutron degeneracy pressure, creating a permanent stellar-mass black hole.
What will SN2026abur's explosion site look like in 1,000 to 10,000 years? Cosmic Remnant
Supernova remnants in general evolve through free-expansion, Sedov–Taylor, and radiative phases over centuries to millennia, sometimes becoming bright X-ray shells and occasionally compressing nearby molecular clouds. These are standard remnant-evolution models, not forecasts measured for SN2026abur. Whether this site will trigger star formation, reach particular X-ray temperatures, or match Cassiopeia A depends on local density and magnetic field—none of which are constrained by the data shown here.
In which galaxy did SN2026abur explode, and where is it located relative to the galactic center? Galactic Environment
No host galaxy is identified for SN2026abur in this catalog record. A blank host field means the association is unresolved here—it does not establish that the host is uncataloged, resolved in imaging, or securely linked by astrometry. Possible states (unidentified, hostless candidate, imaging detection without a catalog name, or a securely matched cataloged galaxy) require separate evidence that is not present in this field.
Where is SN2026abur located in the night sky and which constellation is it in? Sky Coordinates
In the celestial sphere, SN2026abur is located at Right Ascension 01:18:46.498 and Declination +14:59:30.57, situated in the constellation Pisces (The Fishes). Because its declination is +14:59:30.57, it is primarily placed in the Northern celestial hemisphere.
How much Milky Way interstellar dust obscures our view of SN2026abur? Interstellar Dust
Along this line of sight, the catalog records a Milky Way foreground color excess of E(B−V) = 0.0451 mag (source: Analytical Galactic Disk Model (IAU)), corresponding to roughly A_V ≈ 0.14 mag for R_V = 3.1. Band-specific corrections (e.g. A_r) differ from A_V and should be applied when available. Map-based values (IRSA / Schlafly & Finkbeiner 2011) must not be claimed unless that map was actually queried.
Across which photometric filter bands was SN2026abur monitored? Astronomical Observations
SN2026abur was tracked across 11 photometric observations across a baseline of 22.9 days utilizing filter bands including
g, i, i-ZTF, r. Data were captured by observatories and survey networks including ZTF, ZTF, Pan-STARRS, GOTO. Multi-color photometry tracks the temperature evolution of the fireball, verifying the rise time to peak and the rate of radioactive decline.What did astronomical spectroscopy reveal about SN2026abur's chemical makeup? Astronomical Observations
Astronomers obtained 1 spectroscopic epochs for SN2026abur from 3066.0 Å to 10241.0 Å by facilities including P200. Optical spectroscopy provides the definitive physical fingerprint of the transient: P-Cygni line profiles reveal the expansion speed of the ejecta, while characteristic absorption features (such as hydrogen Balmer lines Hα/Hβ in Type II, or Si II λ6355 in Type Ia) identify the stellar composition and physical mechanism of the explosion.
Who discovered SN2026abur and how was it first detected? Discovery & History
SN2026abur was officially reported on 2026/09/14 by ZTFReST_bot. Discoveries are typically flagged by high-cadence robotic survey telescopes (such as ATLAS, ZTF, Pan-STARRS, ASAS-SN, or Gaia) and worldwide amateur astronomers scanning the night sky, followed by rapid spectroscopic classification by international observatories.
How many scientific publications and observatories have contributed data to SN2026abur? Scientific Research
SN2026abur is documented across 4 scientific references and archival data sources in the sne.space. These include discovery circulars and research datasets from Transient Name Server, 2026TNSTR3742....1M, The Open Supernova Catalog, ALeRCE / ZTF. All raw photometry and spectroscopy points are cross-indexed to their original bibliographic records for peer-reviewed verification.
What other names and survey identifiers exist for SN2026abur? Cross-Identifications
Throughout global alert streams and survey databases, SN2026abur has also been designated as:
2026abur, AT2026abur, SN 2026abur, ZTF26abupccs. These cross-matched identifiers allow astronomers to cross-reference observations across the Zwicky Transient Facility (ZTF), the Asteroid Terrestrial-impact Last Alert System (ATLAS), Pan-STARRS, Gaia Photometric Science Alerts, and the IAU Transient Name Server (TNS).How does SN2026abur contribute to measuring the Hubble Constant and the scale of the cosmos? Cosmology & Distance Ladder
As a core-collapse supernova, SN2026abur provides independent cosmological distance calibrations via the Expanding Photosphere Method (EPM) and the Standard Candle Method for Type II supernovae (SCM-II). By correlating the physical expansion speed of the photosphere (measured via spectroscopic Doppler shifts) with its photometric color temperature, astronomers determine direct geometric distances independent of secondary distance ladders.
Could gravitational waves or neutrinos from SN2026abur be detected on Earth? Multi-Messenger Astronomy
Core-collapse supernovae like SN2026abur are premier targets for multi-messenger astrophysics! During the collapse of the iron core, an intense burst of 10⁵⁸ neutrinos escaped into space hours before the shock broke out through the stellar surface (as famously seen in SN 1987A). Furthermore, violent core asymmetries and non-axisymmetric core bounce can emit high-frequency gravitational waves detectable by advanced interferometers (LIGO, Virgo, KAGRA) for events within the Milky Way and Local Group.
How does SN2026abur compare to famous historical supernovae like SN 1987A or the Crab Supernova? Historical Comparison
Compared to historical landmarks like SN 1987A in the Large Magellanic Cloud (168,000 light-years away, naked-eye peak m = 2.9) or the Crab Supernova of 1054 (6,500 light-years away), SN2026abur occurred at a distance of 323.4 Million Light-Years. While historical naked-eye supernovae occurred within our Milky Way or its immediate satellites, modern discoveries like SN2026abur allow astrophysicists to probe diverse galactic environments, metallicities, and stellar populations across the broader universe.
Can I see SN2026abur tonight with a backyard telescope or binoculars? Backyard Observation
Unknown — no measured brightness. SN2026abur was discovered 60 days ago (2026/09/14), but no calibrated photometry is published for it, so its current apparent magnitude cannot be stated. Without a magnitude there is no basis for a telescope-aperture recommendation. Use the coordinates and airmass chart above to plan a follow-up observation and report what you measure.
Does the radiation or shockwave from SN2026abur pose any threat to Earth? Planetary Safety
No, Earth is in zero danger. Supernovae are violent events emitting powerful gamma rays, X-rays, and cosmic rays; however, the astrophysical 'lethal kill zone' for our planet's protective ozone layer is estimated at 50 to 100 light-years. At a distance of 323.4 Million Light-Years, the inverse-square law dilutes the radiation by quintillions of times, making SN2026abur completely harmless to our biosphere and purely a fascinating spectacle for human exploration.
Data sourced from IAU TNS, ALeRCE, WISeREP, and the sne.space.
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